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Energy flows in thick accretion discs and their consequences for black hole feedback

Journal article
Authors A. Sadowski
J. P. Lasota
Marek A Abramowicz
R. Narayan
Published in Monthly Notices of the Royal Astronomical Society
Volume 456
Issue 4
Pages 3915-3928
ISSN 0035-8711
Publication year 2016
Published at Department of Physics (GU)
Pages 3915-3928
Language en
Links dx.doi.org/10.1093/mnras/stv2854
https://gup.ub.gu.se/file/187288
Keywords accretion, accretion discs, black hole physics, relativistic processes, methods: numerical, ADVECTION-DOMINATED ACCRETION, X-RAY BINARIES, MAGNETIC-FLUX, RELATIVISTIC MAGNETOHYDRODYNAMICS, ELECTROMAGNETIC EXTRACTION, DIFFUSION-COEFFICIENTS, NUMERICAL-SIMULATION, GENERAL-RELATIVITY, VERTICAL STRUCTURE, DISKS
Subject categories Astronomy, Astrophysics and Cosmology

Abstract

We study energy flows in geometrically thick accretion discs, both optically thick and thin, using general relativistic, three-dimensional simulations of black hole accretion flows. We find that for non-rotating black holes the efficiency of the total feedback from thick accretion discs is 3 per cent - roughly half of the thin disc efficiency. This amount of energy is ultimately distributed between outflow and radiation, the latter scaling weakly with the accretion rate for super-critical accretion rates, and returned to the interstellar medium. Accretion on to rotating black holes is more efficient because of the additional extraction of rotational energy. However, the jet component is collimated and likely to interact only weakly with the environment, whereas the outflow and radiation components cover a wide solid angle.

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